This study suggests that thermally (at low \(Pr\) ) and mechanically (e.g. tides, precession and libration) driven rotating flows share many features even in the non-linear and turbulent regime, which may have significant implications for some fundamental problems in geophysical and astrophysical fluid dynamics.
Both convection [1]} and mechanical forcings [2]} are thought to be possible driven mechanisms for the generation of Earth's and planetary magnetic fields through the dynamo process. It is possible that dynamos driven by two different mechanisms also share many features in certain parameter regimes and can be studied within the same framework.
In stars and giant planets, the interaction between convection and tides is of great importance for calculating the efficiency of tidal dissipation, yet the problem remains poorly understood [3]}. Turbulent convection is usually treated as an effective viscosity in damping the tidal flow [4]}, [5]}. However, given small \(Pr\)  in the convective zone of rotating stars and giant planets, both convection and tides can drive inertial waves, which would be interacting simultaneously and make it more difficult to estimate the efficiency of tidal dissipation in these systems.
